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REVIEW 4 major objections 8 minor 205 references

Low-mass galaxies at z≈6 follow a steeper mass–metallicity relation than local galaxies, and their UV nitrogen lines reveal globular-cluster-like enrichment.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-01 23:05 UTC pith:WB5I3B46

load-bearing objection Strong new JWST data extend the z~6 MZR to 10^6.6 Msun and show a stacked UV–optical N/O offset, but the steep low-mass slope relies on a Te scale that neglects O+3 and on a calibration fitted to the same stacks. the 4 major comments →

arxiv 2607.15515 v1 pith:WB5I3B46 submitted 2026-07-17 astro-ph.GA

Gas-Phase Metallicity and Nitrogen Abundances in Low-Mass Galaxies Down to M_starsimeq10^(5.7)\,M_odot at zsimeq4.5--10.1 from JWST Lensing Cluster Surveys

Hiroya Umeda , Masami Ouchi , Kimihiko Nakajima , Kuria Watanabe , Yuichi Harikane , Yuki Isobe , Moka Nishigaki , Ono Yoshiaki
show 2 more authors
Hidenobu Yajima Yi Xu
This is my paper
classification astro-ph.GA
keywords mass–metallicity relationgas-phase metallicitynitrogen abundancehigh-redshift galaxiesgravitational lensingstacked spectraWolf–Rayet starsglobular clusters
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper uses 405 deep JWST spectra of gravitationally lensed galaxies at z=4.5–10.1, reaching stellar masses as low as 10^5.7 solar masses, to ask how metals accumulate in the smallest galaxies of the early universe. By stacking spectra in stellar-mass bins and detecting the faint [O III] 4363 auroral line down to a representative mass of about 10^6.6 solar masses, the authors build new empirical strong-line metallicity calibrations and trace the z~6 mass–metallicity relation down to 12 + log(O/H) ≈ 7.2. They find a low-mass slope of 0.38 ± 0.06, steeper than the local value of about 0.28, consistent with efficient metal loss or dilution in shallow gravitational potentials. In the combined stack, the nitrogen abundance inferred from the ultraviolet N IV] doublet exceeds the optical [N II]-based value by about 1.4 dex; together with strong He II 4686 emission, this points to a localized, highly ionized nitrogen-rich component—possibly Wolf–Rayet stars—whose wind nitrogen budget matches the nitrogen excess locked in globular-cluster-like stellar populations.

Core claim

The central discovery is that chemical enrichment in the lowest-mass high-redshift galaxies is both globally ordered and locally diverse. On the global scale, the gas-phase oxygen abundance falls steeply with stellar mass, with a fitted low-mass slope γ = 0.38 ± 0.06 that is steeper than the local relation; the relation reaches 12 + log(O/H) ≈ 7.2 at about 10^6.6 solar masses and matches a range of hydrodynamical simulations. On the local scale, the stacked spectrum at about 10^7.7 solar masses shows N/O from N IV] λλ1483,1486 that is about 1.4 dex higher than N/O from [N II] λ6583, with subsolar C/O and He II 4686/Hβ ≈ 0.03. The authors interpret this as a multi-zone interstellar medium in

What carries the argument

The central machinery is mass-binned stacking of roughly 100 medium-resolution spectra (and about 400 at low resolution), which brings faint diagnostic lines above detection threshold. Metallicities come from the direct method using the [O III] 4363 auroral line under a two-zone ionization model with a fixed relation between low- and high-ionization electron temperatures; the authors then calibrate the R3 ([O III] 5007/Hβ) and R2 ([O II] 3727/Hβ) strong-line ratios against these direct metallicities to extend measurements to galaxies without auroral detections. The mass–metallicity relation is fitted with a turnover function. Nitrogen is measured twice: from the high-ionization UV doublet N

Load-bearing premise

The entire metallicity scale rests on direct-method oxygen abundances that assume a two-zone ionization structure with a fixed electron-temperature relation (low-ionization temperature = 0.7 times high-ionization temperature plus 3,000 K) and neglect O+3; if this temperature or ionization prescription is biased, the calibrations, the mass–metallicity slope, and the N/O comparison all shift together.

What would settle it

Measure [O III] 88 µm together with [O III] 5007 in a magnified galaxy with stellar mass near 10^6.6 solar masses at z~6: the far-infrared line gives an independent electron temperature and oxygen abundance. A value of 12 + log(O/H) more than about 0.3 dex above 7.2 at that mass would flatten the low-mass slope. Alternatively, a single high-signal-to-noise spectrum with auroral-line temperatures from both [O III] 4363 and [O II] 7325 that disagrees with the assumed two-zone temperature relation would force recalibration.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • If the steep slope holds, the smallest galaxies at z~6 lose or dilute most of their metals, so their interstellar oxygen abundances sit roughly ten times below local galaxies of the same mass.
  • The new empirical strong-line calibrations can be applied to faint JWST samples without auroral lines, extending metallicity measurements to mass regimes that are otherwise inaccessible.
  • The systematic disagreement between UV and optical nitrogen diagnostics in the same systems means abundance interpretations based on only one spectral window are incomplete; each window traces a different gas phase.
  • Nitrogen overabundance seen in bright individual galaxies is also present in stacked low-mass populations, making it a common enrichment mode rather than a rare anomaly.
  • The comparable nitrogen mass in stellar winds and in globular-cluster enriched populations points to a concrete channel by which early, compact star formation could seed the abundance patterns seen in ancient star clusters.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the multi-zone reading is right, single-zone N/O values in the literature that rely on UV lines alone are likely biased high by bright, N-rich clumps; correcting for this could bring many high-redshift nitrogen emitters back onto the local N/O–O/H sequence.
  • The same stacks could test the Wolf–Rayet hypothesis directly: medium-resolution spectroscopy of individual magnified clumps in z~6 lensed arcs should show whether N IV] and He II peak on globular-cluster-scale regions while [N II] traces the surrounding diffuse gas.
  • A prediction of the enrichment-burst picture is that metallicity and N/O should vary stochastically with star-formation history; comparing these stacks with simulations that track 10-million-year bursts could discriminate prompt Wolf–Rayet enrichment from delayed AGB winds.
  • The empirical calibration approach could be extended to C/O and Ne/O as functions of stellar mass, giving a two-element clock for the onset of enrichment in the lowest-mass galaxies.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

4 major / 8 minor

Summary. Umeda et al. analyze 405 JWST/NIRSpec spectra of gravitationally lensed star-forming galaxies at z=4.5–10.1 from the DREAMS, GLIMPSE-D, GLASS, ERO, SPURS, UNCOVER, and CANUCS programs, with 50% of the M_UV>−17.5 sources magnified by μ>3. They construct stellar-mass-binned stacks (GM1–GM4, GAll and prism-resolution analogs), detect [OIII]λ4363 down to a representative stellar mass of ~10^6.6 M⊙, and derive direct-method oxygen abundances using a two-zone Te scheme (Eqs. 3–4). They fit new empirical R3/R2 strong-line calibrations (§4.4.2) to the direct-method stack metallicities, individual auroral-line detections, and local analogs, then apply them to trace the z~6 MZR to M*≈10^6.6 M⊙, fitting a Zahid et al. (2014) form with low-mass slope γ=0.38±0.06 (Table 6), reported as slightly steeper than the local γ≈0.28. In the GAll stack (M*≈10^7.7), the Niv]-based [N/O] is 0.66±0.24, ~1.4 dex above the [Nii]-based value (−0.73±0.11); with subsolar C/O and HeII λ4686/Hβ≈0.03, this is interpreted as a multi-zone ISM containing a localized, N-rich, globular-cluster-like component, with an order-of-magnitude estimate suggesting that a WNE-like stellar population could supply the required nitrogen mass.

Significance. The compiled lensing sample and the stacking products are a valuable community resource: the MZR baseline is extended two decades below previous z~6 measurements, the [OIII]λ4363 detection at M*≈10^6.6 M⊙ is a technically demanding result, and the tabulated empirical (Table 6) and photoionization-model (Table 7) calibrations are directly usable. The UV–optical N/O comparison in an average low-mass galaxy, if secure, would strengthen the case that nitrogen enhancement is widespread at high redshift and connect early enrichment to globular-cluster abundance patterns. These strengths are real, but the headline claims are currently anchored on a partly circular calibration, an unquantified O+3 systematic on the Te scale, and ~3σ line detections. The good news is that each of these can be quantified or tested with the authors' own model grids and robustness fits; the manuscript does not currently do so.

major comments (4)
  1. [§4.4.2, §4.5, Eq. (7), Fig. 10] The new R3/R2 calibration is fitted using the direct-method metallicities of the same GM1–GM4 grating stacks (plus individual auroral-line detections and Andrews & Martini 2013 analogs) that are then used to construct the empirical MZR. The agreement between the direct and empirical methods shown in Fig. 10 is therefore partly by construction for the stacks, and the claim in §4.4.2 that this agreement 'demonstrates the internal consistency of the calibration' overstates the validation. The empirical MZR does not independently confirm the direct-method MZR; both trace the same Te-scale anchors. Please report the stack residuals in the calibration fit and perform a leave-one-stack-out cross-validation, so the reader can see how well the calibration predicts a stack excluded from the fit.
  2. [§4.4.1, Eq. (4), Table 4, §5.1] Eq. (4) sums only O+ and O+2, and the paper notes (end of §4.4.1) that neglecting O+3 'may introduce a systematic uncertainty for systems with hard ionizing spectra' — exactly the regime probed here: HeII λ4686/Hβ≈0.03 (Table 3) and O32≳15 in GM1, decreasing to ≈4 in GM4 (Table 4). If a non-negligible O+3 fraction is present in the low-mass stacks, the direct-method O/H values are underestimated; because O32 is strongly mass-dependent, the bias is mass-dependent and will tend to steepen the fitted low-mass slope γ=0.38±0.06. A +0.1–0.2 dex correction at the GM1–GM2 end would bring the slope to the local value within the quoted uncertainty; the current ~1.7σ difference from the local γ≈0.28 is not robust to this systematic. Please quantify O+3/O using the paper's own Cloudy model grids (Appendix A) at the observed O32, C43, and HeII strengths, and quote γ with and without the correction.
  3. [Table 2, Table 4, §4.5] The two lowest-mass anchors are fragile. (i) GM1's [OIII]λ4363/Hβ=0.12±0.04 is a ~3σ detection, at the adopted stack threshold; its direct-method oxygen abundance (12+log(O/H)=7.27^{+0.21}_{-0.14}) carries this statistical fragility into the MZR fit. (ii) GM1's [OII] is a 3σ upper limit (<0.21), so R2 is not measured, yet the quoted empirical metallicity uncertainty for GM1 (7.27±0.06) is smaller than the direct-method uncertainty and it is unclear how the upper limit enters the likelihood of Eq. (6). Because GM1 is the point that controls the difference between γ=0.38 and the local γ≈0.28, the paper should show the MZR refit with GM1 excluded and state explicitly how upper limits are propagated in Eq. (6).
  4. [§4.6.1, Table 3, Appendix A] The claimed 1.4-dex discrepancy between [N/O]UV=0.66±0.24 and [N/O]Opt=−0.73±0.11 rests on the Niv] λλ1483,1486 detection in GAll at S/N≈3 (flux 0.12±0.05; the stack detection criterion is S/N≥3), and on a photoionization-model ionization correction whose AGN variant shifts the Niv]/Oiii] calibration by ≈0.2 dex (Table 7). Please report the achieved S/N of Niv] explicitly, propagate the spread among the stellar, AGN, and WNE calibrations (Table 7) into [N/O]UV, and state how the significance of the 1.4-dex offset is affected once this model systematic is included. As written, the statistical and model uncertainty budget is not sufficient to establish the discrepancy quantitatively, even though the direction of the offset is consistent with literature results.
minor comments (8)
  1. [§4.2, Table 6] The fitted O32 relation is printed as logO32 = −0.243±0.004 + (2.89±0.27) log(M⋆/M⊙). As written this has the wrong sign/roles: it predicts O32 increasing steeply with stellar mass, contradicting the text ('higher ionization parameter at lower stellar mass') and Fig. 7; the intended relation is logO32 ≈ 2.89 − 0.24 log(M⋆/M⊙) (with the coefficients interchanged and b1 negative). Since this relation is used to infer R2 in Eq. (6), the printed formula must be corrected for reproducibility.
  2. [Table 4] The O32 column lists linear ratio values (e.g., 12.86^{+2.17}_{-1.47} for GM2 and the lower limit >15.01 for GM1) while §4.2 and Fig. 7 work in log space. Please state units in the column header and mark GM1's entry explicitly as a lower limit throughout (as done in Table 2 for [OII]).
  3. [§4.5, Table 6] The MZR is fit to four stack points with three effective free parameters (β fixed at 49). Report the covariance among Z0, logM0, and γ, and add the 0.07–0.08 dex RMS of the strong-line calibration (Table 6) and Te-scale systematics to the quoted γ uncertainty. The abstract's 'slightly steeper' is appropriately cautious, but Summary item 2 ('steep low-mass-end slope... sharp decrease') is stronger than justified by a ~1.7σ difference from the local γ≈0.28.
  4. [§2.5–§4.5] The sample spans z=4.5–10.1 and the MZR is labelled z~6. Please state the median redshift of each stack (GM1–GM4, GAll) to quantify the epoch over which each stack is averaged; a ~1-Gyr baseline could introduce redshift-evolution scatter into the stacked MZR.
  5. [Tables 2–3] Please report the achieved S/N for the marginal detections ([OIII]λ4363 in GM1, Niv] in GAll, [NII]λ6583 in GAll) in the tables, since the stacked criterion is S/N≥3 and several values sit at or near this boundary.
  6. [§2.1.1] The DREAMS data reduction is described as 'forthcoming (Nakajima et al., in preparation)'. For reproducibility, cite the public data products or the companion pipeline paper, and provide the same for the other survey reductions where available.
  7. [Throughout] Typographical issues: 'T able' (Table 1 caption); 'W AIC'/'∆W AIC' (§2.3); inconsistent 'Wolf-Rayet' vs 'Wolf–Rayet'; 'Hβflux' missing space (§3); corrupted symbol 'λW4686' in the abstract; 'D WN' in the Acknowledgments; 'MAG AUTO' should be MAG_AUTO; mass-loss units 'M⊙ yr−1' are missing after Ṁ in §5.3.
  8. [Introduction, References] The Introduction cites 'A. J. Cameron et al. 2023' for high-z nitrogen enhancement; the widely used reference for a nitrogen-enhanced galaxy at z~5–7 is Cameron et al. 2024 (Nature). Please verify the intended citation and that the reference list entries ('Cameron et al. 2023' and 'Cameron et al. 2026') correspond to the claimed results.

Circularity Check

1 steps flagged

The empirical-calibration MZR for the stacks re-states the same direct-method O/H values the calibration was fitted to; the steep low-mass slope is not an independent strong-line prediction, though the direct-method MZR gives some independent support.

specific steps
  1. fitted input called prediction [Section 4.4.2 (Strong-Line Calibrations), Section 4.5 (Mass–Metallicity Relation), Eq. (7), Table 6, Figs. 9–10]
    "Instead of adopting a calibration from the literature, we derive empirical relations between the strong-line ratios and direct-method metallicity ... The fit uses our grating stacked spectra and individual measurements with auroral-line detections. ... Based on the newly derived calibration, we derive strong-line based empirically calibrated metallicities ... for individual galaxies and stacked spectra using the observed R3 and R2 values. ... We fit the MZR using the stacked spectra metallicity measurements based on the empirical calibration."

    The R2/R3 calibration is fitted to direct-method 12+log(O/H) values of the same grating stacks (GM1–GM3) and individual galaxies with [OIII]4363 detections. Those same stacks are then assigned 12+log(O/H)_Emp by inverting that calibration, so their empirical metallicities coincide with the direct-method inputs to within the polynomial fit residuals (Fig. 10). Fitting the MZR (Eq. 7) to these empirical stack values therefore makes the resulting low-mass slope gamma=0.38+/-0.06 a smoothed re-statement of the direct Te-based O/H of the same bins, not an independent strong-line prediction. GM1 is additionally self-referential: [OII] is a non-detection, so R2 is imported from the O32–M* relation fitted on the same stacks, making the lowest-mass anchor twice dependent on its own direct-method va

full rationale

The identifiable circular step is confined to the empirical strong-line calibration pipeline. The paper explicitly fits the calibration to direct-method metallicities of the grating stacks and then uses the empirically calibrated metallicities of those same stacks to fit the MZR; for GM1–GM3 the empirical values are, by construction, close to the input direct-method values. Therefore the advertised 'empirical calibration' MZR for the stacks is not an independent confirmation of the direct-method result. The paper does, however, also present a direct-method MZR (Fig. 12) that is independent of the calibration itself, and the direct Te measurements are not derived from the strong-line calibration. So the steep low-mass slope is not wholly manufactured; it inherits whatever systematic biases are in the Te method (e.g., the assumed Te([OII])–Te([OIII]) relation and neglected O+3), which is a correctness/robustness concern rather than circularity per se. No load-bearing self-citation or uniqueness-imported-from-authors pattern was found; self-citations to Isobe, Nakajima, Ouchi, and other (partly overlapping) works are methodological and do not by themselves force the conclusions. Score 5 reflects one genuine partial circularity in the empirical-calibration MZR, with the central claim still retaining independent direct-method content.

Axiom & Free-Parameter Ledger

4 free parameters · 8 axioms · 1 invented entities

The central measurements rest on standard JWST reduction and SED fitting, plus a newly derived strong-line calibration that is partly fitted to the same stacked spectra it calibrates; the N/O and WR/GC interpretation adds adopted stellar-atmosphere and globular-cluster parameters.

free parameters (4)
  • MZR fit parameters (Z0, logM0, gamma, beta) = Z0=8.06±0.09, log(M0/Msun)=8.85±0.31, gamma=0.38±0.06, beta=49
    Fitted to stack metallicities in Eq. 7; beta poorly constrained and effectively fixed, so the low-mass slope is the main fitted quantity.
  • Strong-line calibration coefficients (c0,c1,c2 for logR3 and logR2) = logR3: 0.0680, 1.8282, -1.0690; logR2: -1.2276, 1.7359, -0.3747
    Polynomial coefficients fitted to direct-method metallicities of grating stacks, individual auroral detections, and Andrews & Martini (2013) analogs.
  • Stellar-mass–line-ratio relations (logO32, logC43) = logO32 = -0.243 + 2.89 logM; logC43 = -0.60 + 4.33 logM
    Used to infer R2 and C43 for sources without [OII] coverage and for abundance calibrations; fitted to the stacks.
  • WNE/GC mass-budget assumptions = N_WN~1650, t_WNE=0.5 Myr, X_N=1.5e-3, f_enriched=0.7, [N/H]_enriched=-0.7, M_GC=2e5 Msun
    Hand-adopted values in the order-of-magnitude estimate linking HeII and nitrogen wind mass to globular-cluster excess.
axioms (8)
  • domain assumption Te([OII]) = 0.7 Te([OIII]) + 3000 K
    Empirical relation from Campbell/Garnett used for all direct-method O/H; §4.4.1.
  • domain assumption Two-zone ionization model neglecting O+3
    O/H from O+ and O+2 only; O+3 contribution could bias metallicities; §4.4.1.
  • domain assumption Electron density adopted from Topping et al. (2025) redshift relation
    Used for abundance calculations rather than per-stack measured densities; §4.3.
  • domain assumption BPASS v2.2.1 + Cloudy grids and Calzetti attenuation for SED fitting
    Stellar masses and SFRs from Bagpipes; §2.4.
  • domain assumption Photoionization abundance calibrations assume plane-parallel, constant-density clouds with solar relative abundances
    N/O, C/O, Ne/O, Ar/O inferred through offsets from solar-pattern model sequences; Appendix A.
  • domain assumption Lensing magnification models are correct
    Absolute UV magnitudes and derived stellar masses depend on glafic/UNCOVER/CANUCS lens models; §2.2.
  • ad hoc to paper WNE parameters (logT*=5.25, Mdot=1.2e-5 Msun/yr, M*=12 Msun)
    Adopted PoWR SMC WNE model used to estimate N_WN and nitrogen wind mass; §5.3.
  • ad hoc to paper Globular-cluster enrichment parameters (f_enriched=0.7, [N/H]_enriched=-0.7, M_GC=2e5 Msun)
    Order-of-magnitude comparison of nitrogen mass; §5.3.
invented entities (1)
  • WNE-like stellar population component beyond BPASS no independent evidence
    purpose: Explains HeII 4686/Hbeta~0.03 and the UV nitrogen excess with ~1650 WNE-like stars contributing ~10% of Hbeta
    Phenomenological component introduced in §5.3; its existence is inferred from the same line ratios it is meant to explain, and the paper explicitly cautions it is not a simple addition of ordinary WR stars to BPASS.

pith-pipeline@v1.3.0-alltime-deepseek · 44574 in / 17005 out tokens · 168902 ms · 2026-08-01T23:05:41.304294+00:00 · methodology

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read the original abstract

We analyze 405 deep JWST/NIRSpec spectra of star-forming galaxies at $z=4.5$--$10.1$ from DREAMS and other lensing-cluster surveys to study chemical enrichment in intrinsically faint, low-mass galaxies. The sample covers $M_{\rm UV}\simeq-12$ to $-22$ and reaches $M_\star\simeq10^{5.7}\,M_\odot$, with 50\% of the sources at $M_{\rm UV}>-17.5$ magnified by $\mu>3$. From individual spectra and mass-binned stacks, we derive the gas-phase metallicity together with nitrogen and carbon abundances using the rest-frame UV and optical lines. \Add{We derive new empirical strong-line metallicity calibrations using direct-method measurements from stellar-mass-binned stacks, reaching a representative stellar mass of $M_\star\simeq10^{6.6}\,M_\odot$. Applying these calibrations, we trace the $z\sim6$ mass--metallicity relation down to $M_\star\simeq10^{6.6}\,M_\odot$, where it reaches $12+\log({\rm O/H})\simeq7.2$, with a low-mass slope slightly steeper than the local relation and in broad agreement with hydrodynamical simulations.} In the $M_\star\simeq10^{7.7}\,M_\odot$ stack, N/O from N\,{\sc iv}]\,$\lambda\lambda\,1483,1486$ exceeds that from [N\,{\sc ii}]\,$\lambda6583$ by $\simeq1.4$ dex. The UV--optical difference could indicate a localized, highly ionized N-rich component whose high N/O and subsolar C/O resemble nitrogen-rich globular-cluster populations with $M_\star\lesssim10^6\,M_\odot$. \Add{The combination of these abundance patterns and a He\,{\sc ii}\,\W4686/H$\beta$ ratio of $\simeq0.03$, well above BPASS predictions, suggests that WR stars may contribute both prompt CNO-cycle enrichment and hard ionizing radiation, with the inferred WR population potentially supplying enough nitrogen to account for the excess on globular-cluster scales.

Figures

Figures reproduced from arXiv: 2607.15515 by Hidenobu Yajima, Hiroya Umeda, Kimihiko Nakajima, Kuria Watanabe, Masami Ouchi, Moka Nishigaki, Ono Yoshiaki, Yi Xu, Yuichi Harikane, Yuki Isobe.

Figure 1
Figure 1. Figure 1: The distribution of UV magnitude by redshift for the sample after excluding AGN and LRD candidates. Cir￾cles and crosses correspond to the objects at z < 8 (z > 8) with F150W (F200W) band detection or non-detection, re￾spectively. For the non-detection sources, we present the 3σ upper limit. The colors indicate the magnification factor, with the color bar at left showing the corresponding scale [PITH_FULL… view at source ↗
Figure 2
Figure 2. Figure 2: The BPT diagram. The objects encircled by blue diamonds, red circles, and yellow pentagons represent the AGN candidate selected from the broad line detection (Type-I AGN candidate), BPT selection, and red optical slope (i.e., LRD candidates). 2.5.1. Sample Selection To mitigate AGN contamination, we exclude galax￾ies showing AGN-like line ratios using the classical BPT diagram based on [O iii]/Hβ and [N ii… view at source ↗
Figure 3
Figure 3. Figure 3: The stacked spectra of the full star-forming galaxy sample at grating (GAll) and prism (PAll) resolutions are shown in the top and bottom panels, respectively. For both the GAll and PAll spectra, the UV (left) and optical (right) components are arbitrarily normalized for visualization. The wavelengths of key emission lines are marked by vertical dotted lines. The shaded regions indicate the 1σ uncertaintie… view at source ↗
Figure 4
Figure 4. Figure 4: Zoomed-in stacked spectra around key UV and optical emission lines, including C iv λλ1548,1551, C iii] λλ1907,1909, [O ii] λλ3727, 3729, Hγ+[O iii] λ4363, Hβ+[O iii] λλ4959, 5007, Hα, and [S ii] λλ6716,6731. The spectra are shown in the rest frame and are arbitrarily scaled for visualization. The grey hatched regions indicate the 1σ uncertainties estimated through bootstrap resampling. The vertical dotted … view at source ↗
Figure 5
Figure 5. Figure 5: Zoomed-in GAll stacked spectra around key optical and UV emission lines. The left panel shows the UV spec￾tra around N iv] λλ1483, 1486, C iv λλ1548, 1551, He ii λ1640 + O iii] λλ1661, 1666, the N iii] λ1750 quintet, Si iii] λλ1883, 1892, and C iii] λλ1907, 1909. The right panel shows the optical spectra around [O ii] λλ3726, 3729, Hγ+[O iii] λ4363, Hβ + [O iii] λλ4959, 5007, and Hα + [N ii] λλ6548, 6583. … view at source ↗
Figure 7
Figure 7. Figure 7: Stellar-mass dependence of (a) O32 and (b) C43. In panel (a), the solid black dots represent indi￾vidual galaxies with detections of [O ii] λλ3726, 3729 and [O iii] λλ4959, 5007, while the transparent black dots rep￾resent galaxies with non-detections of [O ii] λλ3726, 3729. In panel (b), the solid black dots represent individ￾ual galaxies with detections of C iv λλ1548, 1551 and C iii] λλ1907, 1909, while… view at source ↗
Figure 8
Figure 8. Figure 8: Electron density inferred from the [S ii] λλ6716,6731 and C iii] λλ1907,1909. The turquoise and orange symbols represent the electron density measurements based on the [S ii] and C iii] ratios as a function of stellar mass, respectively. The squares and stars represent the measurements from the stacked spectra for each stellar mass bin (i.e., GM1 to GM4) and the all-galaxy stacked spectrum (i.e., GAll), re… view at source ↗
Figure 9
Figure 9. Figure 9: Empirical calibrations between strong-line ratios and direct-method metallicity. (a) The relation between R3 and 12 + log(O/H). (b) The relation between R2 and 12 + log(O/H). The red squares and black circles represent measurements from our grating stacked spectra and individual galaxies with auroral-line detections, respectively. The white crosses represent measurements from the stacked spectra of local h… view at source ↗
Figure 10
Figure 10. Figure 10: The comparison between the gas-phase metal￾licities measured from the direct method and the empirical strong line relations. The black dots represent the measure￾ments for the grating galaxy spectra with [O ii] λλ3726, 3729, [O iii] λ4363, Hβ, and [O iii] λλ4959, 5007 detections. The red squares represent the measurements for the stacked spec￾tra from the grating sample. The gray dashed line corre￾sponds … view at source ↗
Figure 11
Figure 11. Figure 11: The stellar-mass and gas-phase metallicity relation (MZR) at z ∼ 6 (i.e., z ≃ 4.5 − 9) based on the strong line calibrations. The black circles represent the measurement from individual galaxies with Hβ or [O iii] λλ4959,5007 detections. The large red squares represent the measurements from the stacked spectra from the grating sample in each stellar-mass bin. The gray dots represents the measurement from … view at source ↗
Figure 14
Figure 14. Figure 14 [PITH_FULL_IMAGE:figures/full_fig_p019_14.png] view at source ↗
Figure 13
Figure 13. Figure 13: The comparison between the MZR measure￾ment based on the R ∼ 1000 stacked spectra (red circles), R ∼ 100 stacked spectra (turquoise squares), and the binned measurements from individual galaxies (grey diamonds). the physical assumptions and the other observables such as chemical abundances. 5.2. The Origin of Chemical Enrichment To understand the physical origin of the chemical en￾richment in the galaxies… view at source ↗
Figure 15
Figure 15. Figure 15: (a) The [N/O] abundance ratio derived using N iv] λλ1483,1486 and O iii] λλ1661,1666 as a function of stellar mass. The red star represents our measurement for the GAll stack. The grey, blue, and red symbols correspond to the measurements for z ∼ 0 (Z. Martinez et al. 2025), 1–4.5 (B. Welch et al. 2025), and > 4.5 (Y. Isobe et al. 2023b; M. Castellano et al. 2024; D. A. Berg et al. 2026; M. Curti et al. 2… view at source ↗
Figure 16
Figure 16. Figure 16: (a) The [N/O] abundance ratio derived using N iv] λλ1483,1486 and O iii] λλ1661,1666 as a function of gas-phase metallicity. The red star represents the our measurement for GAll stack. The grey, blue, and red symbols correspond to the measurements for z ∼ 0 (Z. Martinez et al. 2025), 1–4.5 (B. Welch et al. 2025), and > 4.5 (Y. Isobe et al. 2023b; M. Castellano et al. 2024; D. A. Berg et al. 2026; M. Curti… view at source ↗
Figure 17
Figure 17. Figure 17: (a) The [C/O] abundance ratio derived using UV spectra as a function of stellar mass. We show the measurements of the z ∼ 2 galaxies from D. A. Berg et al. (2019) in grey diamonds and the literature z > 6 N-enhanced galaxies in red diamonds (e.g., Y. Isobe et al. 2023b; K. Z. Arellano-C´ordova et al. 2025; X. Ji et al. 2024; D. Schaerer et al. 2026). The grey horizontal band represents the C/O yield from … view at source ↗
Figure 18
Figure 18. Figure 18: The mass–metallicity relation from the simula￾tions with different ISM assumptions. The blue solid, orange dashed, purple dotted, and yellow dotted-dahsed lines repre￾sent the mass–metallicity relation predictions by the Fire-2 (A. Marszewski et al. 2024), FirstLight (I. Langan et al. 2020), Serra (A. Pallottini et al. 2025), and Thesan-zoom (W. McClymont et al. 2026) simulations, respectively. The black … view at source ↗
Figure 19
Figure 19. Figure 19: The [C/O]UV vs. [N/O]UV abundance ratio. The red star represents the measurements for the stacked spectra from all galaxy grating spectra. The other red symbols represent the abundance measurements of N iv] emitters from literature. The gray solid line corresponds to the best-fit relation for the local H ii regions from the GCE model for Milky Way from C. Kobayashi et al. (2020). Cyan, olive, and blue sol… view at source ↗
Figure 20
Figure 20. Figure 20: (Top): The [N/O] vs. [Ar/O] and [N/O] vs. [Ne/O] abundance ratios. (Bottom): The [C/O] vs. [Ar/O] and [C/O] vs. [Ne/O] abundance ratios. For GAll, Ar/O is a 1σ upper limit, indicated by the leftward arrows, whereas Ne/O is a measurement. The symbols are otherwise the same as in [PITH_FULL_IMAGE:figures/full_fig_p024_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: Comparison of the observed He ii λ4686/Hβ ra￾tio with the maximum values predicted by the BPASS, AGN, and WNE models as a function of C43. The observed value is shown by the yellow star, while the shaded regions extend￾ing up to the model maxima represent BPASS (black), AGN (red), and WNE (turquoise). For the model descriptions, see Appendix A. (2024) proposes the stratified multi-zone ISM to explain the … view at source ↗
Figure 22
Figure 22. Figure 22: The [N/O] abundance ratio as a function of (a) stellar mass and (b) gas-phase metallicity. The red and gray symbols represent UV- and optical-based N/O measurements, respectively, from this work and the literature samples compiled in Figures 15 and 16. The red and gray stars show the corresponding measurements for GAll. The turquoise symbols represent stellar-abundance measurements of globular-cluster mem… view at source ↗
Figure 23
Figure 23. Figure 23: Photoionization-model relations between C iv/C iii] and the abundance-sensitive N iv]/O iii], C iii]/O iii], [Ar iv]/O iii], and [Ne iii]/O iii] emission-line ratios. All models use a plane-parallel, constant-density cloud with solar rela￾tive abundances and span −3 ≤ log U ≤ 0 and log(ne/cm−3 ) = 1, 3, and 5. Colors show the ionization parameter, electron density, and input radiation field. The radiation… view at source ↗

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